Although the stellar signal significantly impacts the detection and characterization, RVs have been widely used to detect exoplanets, especially for low mass planets [1]}.
These low mass and/or long period planets induce RV semi-amplitudes similar to or smaller than those produced by stellar activity [2]}, [3]}, [4]}. Therefore, it is highly important to put effort in understanding and correcting for stellar activity, as it is essential for accurate RV detection and hence for characterizing interesting new exoplanets.
Instrument stability is no longer the dominant obstacle for the precise and accurate mass determination of low-mass planets orbiting bright stars, considering the advanced latest generation of instruments. However, it is often limited by the intrinsic stellar variability [5]}, [6]}, [7]}. So, caution is needed while characterizing planets discovered with the RV method around stars that are active/potentially active, as this method is highly prone to the uncertainty arising from the host star's activity.
